| Start Date | Context | Status | Description |
|---|---|---|---|
| 2026-04-20 | hst_1328.pmap | latest | Delivery of new STIS CCD bias and dark reference files for CCD data taken between March 17 2026 through April 16 2026. The files were generated from data taken in the same time frame under STIS calibration programs 18157 and 18155. |
| 2026-04-17 | hst_1327.pmap | archived | These WFC3 UVIS superdarks will affect all UVIS data taken from March 2, 2026 to March 30, 2026. Currently, the automated calibration pipeline and CRDS have only WFC3 UVIS drk and dkc reference files with USEAFTER dates of up to February 28, 2026. The automated pipeline should now use these reference files to perform dark subtraction on any UVIS datasets obtained between the dates above, as they represent the most accurate picture of dark current and hot pixels for this time period. These WFC3 UVIS drk and dkc files were generated using dark exposures from HST Cycle 33 CAL programs 17944, 17946, and 17947. More information regarding the method used to create the UVIS dark calibration reference files can be found in WFC3 ISR 2016-08. Additionally, the header of each reference file contains a detailed history section outlining the process, and provides a list of data used to create each file. This new bad pixel table with USEAFTER of March 2, 2026 was generated using data taken from March 3, 2026, through April 2, 2026. Currently, the Calibration Reference Data System only has WFC3 UVIS bad pixel reference tables up to a USEAFTER date of February 2, 2026. The automated pipeline should now use this reference file as the bad pixel table on any UVIS datasets obtained from March 2, 2026 to present because it represents the most accurate measure of pixel stability at the time of the science observation. These WFC3 UVIS bad pixel files were generated using 900 second dark exposures from the HST Cycle 33 daily monitoring programs 17944, 17946, and 17947. More information about the UVIS bad pixel tables is outlined in the WFC3 ISR 2018.15 and WFC3 ISR 2021.14. |
| 2026-04-13 | hst_1324.pmap | archived | The ACS WFC bias, dark, CTE dark, and sink files were generated following the ACS WFC anneal on April 7, 2026, and should be used to calibrate ACS WFC observations taken between March 10, 2026 and April 7, 2026. |
| 2026-04-08 | hst_1323.pmap | archived | A new ACS WFC post-flash reference file, FLSHFILE, is being delivered because new post-flash calibration data was taken in Nov 2025 as part of proposal 17986. The raw darks were separated by EXPTIME and FLASHDUR and combined with ACSREJ to create short and long-flashed superdarks. These superdarks were differenced and scaled to create an intermediate data product that was then smoothed with a local median filter and renormalized to produce the final post-flash reference file. This reference file is to be used in the calibration of ACS WFC post-flashed data taken after July 01 2025. |